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Dust effects in the SEDs of simulated gala the GRASIL-3D code and some applicatio Rosa Domínguez-Tenreiro Universidad Autónoma de Madrid, Spain A. OBREJA (UAM, Spain) G.L. GRANATO (INAF, Trieste, Italy) I. SANTOS (UAM, Spain) C. A. BROOK (UAM, Spain) G. STINSON (MPIA, Heidelberg, Germany) L. SILVA (INAF, Trieste, Italy) A. SERNA (UMH,Spain) S. GOTTLOBER, Y. HOFFMAN, G. YEPES & CLUES Collaboration Dust Effects in galaxy SEDs Galaxy formed in a hydro simulation Z=6 t/t_U=0.066 DECREASING UV optical // INCREASING IR submm L DUST reradiates the overall bolometric luminosity SED has been calculated with GRASIL3D code (D-T et al, 2014) Simulations: information on 6D phase space, ages, composition, gas density and temperature. Observations: light Testing simulations (theories & models) against observations demands SOFTWARE TELESCOPES: Simulation outputs ----> SEDs, images DUST EFFECTS: FUNDAMENTAL ROLE in GALAXY SEDs GRASIL-3D Application I.- Testing G-3 local galaxies Application II.- IR-submm emission from CLUES Local Group dwarfs Application III.- The MS and the Fundamental Plane of star-forming galaxies GRASIL-3D: An extension of GRASIL to arbitrary geometries and galaxy evolutionary histories (D-T+ 14) RADIATIVE TRANSFER THROUGH DUST SUNRISE (Jonsson 04,05; +09) RADISHE (Chakrabarti+08; & Whitney09) ART2 (Li + 07; Yajima+12) MCarlo solve RT for Simu outputs GRASIL assumes Equatorial & axial symmetry for galaxies SAMS PEGASE (Fioc & Rocca-Volmerage 1997) CIGALE (Burgarella + 14) Parameter determination SKIRT (Baes+ 03, 11) GRASIL(-3D) PARTICULARITIES Separately treats RT in MCs and in cirrus, different dust composition Age-dependent dust reprocessing of stellar populations: younger *s in denser ISM embeded in MC until destruction Detailed non-equilibrium calculation for dust grains with diameter a < 250 A ---> Proper PAH treatment RT solved in a grid, rather than MCarlo CHARGE VARIABLES to a GRID MC & CIRRUS DISTRIBUTION Based on sub-resolution PDF (Wada+07 ; Federrath + 12) Choose a density threshold for MC rho_thres Choose a 2 parameter log-normal PDF for the cold gas f_pd(rho_0, sig) For the ith particle Identify <rho>_V = rho_gas(i) (**) → Calculate the MC mass fraction at ¨i¨ Calculate cirrus mass fraction at ¨i (**) provides a link between PDF parameters and simulation outputs ---> PDF sig AGE DEPENDENT DUST REPROCESSING OF SP Light fraction that can escape the StarBurst region, mimicking MC destruction, f(t) = 1 if t<t_0 0 if t>2t_0 2-t/t_0 in other cases DUST CONTENT k-th GAS PARTICLE d(Z_k) = Z_gas,k /(110 x Z_sun) PARAMETERS GRASIL 3D Grid size simulation resolution rho_mc,thres 10 – 100 H/ cm^3 (Obs + simu) 1 PDF parameter sig 2 – 3 in simulations ---> cirrus & MC mass fraction f_mc GRASIL Dust model Escape-time-scale t_0 2.5-8 or 18-50 Myrs (N,SB) Individual MC log(m_mc) = 5 -6 M_o; r_mc= 10-50 pc SIMULATION: SHAPE, EVOLUTION MODEL, SFRH I TESTING GRASIL-3D LOCAL GALAXIES SIMULATIONS P-DEVA AP3M-SPH Entropy conserving; mutual neighbors (Martínez-Serrano+ 08) OK Chemical evolution tracks the full dependence of metal production on the detailed chemical composition of * particles (Q_ij formalism, Talbot+ 73) Feedback: implicitely through (inefficient) SF parameters (Agertz+ 11) GASOLINE SPH (Wadsley + 04,Brook + 11) Feedback: blastwave formalism (Stinson+ 06) from Sne & massive stars (Stinson+ 13). Effective coupling with gas 1% Blast-wave scenario Face- and edge on images of g1536_L* Box 50 kpc side, resolution and pixel = 312,5 pc OBSERVATIONAL SAMPLES GRASIL-3D TESTING ISO Key Project on the ISM of Normal Galaxies ISO & IRAS broad-band fluxes FIR active, quiescent and intermediate (Vega+05) Helou+96; Dale+ 00 Aromatic Features in Emission 6.2,7.7,8.6 & 11.3 micron (Lu+03; a subsample of Dale+00) Spitzer IR Normal Galaxy Survey (SINGS ; Kennicutt+03; Dale+05) Non-tidally perturbed & non-interacting galaxies (Smith+07, a SINGS subsample & Lanz+13 from KINGFISH) Key Insights on Nearby Galaxies: FIR Survey w Herschel (KINGFISH, Kennicutt+11) All normal types 61 galaxies imaged with PACS and SPIRE (Dale+12) MOLECULAR and ATOMIC HYDROGE & STELLAR CONTENT A test for the MC model in GRASIL-3D Simulations vs COLD GASS survey (Saintonge+11) OK IRAS flux density ratios: simulated (color) vs real (Gray: Dale+00) galaxies LEFT: Merger RIGHT: Normal FIR active, quiescent and intermediate (Vega+05) Lines join consecutive results for HD-5103B along a merger phase AFE Rel Strengths vs FIR/blue At z=0 and around a MM Gray points: data Lu+03 FIR-active,intermediate,quiescent Color: simulations 8 gal. z=0 BLUE And merger phase Different parameter Sets Codes as in previous Fig.left Observational results recovered Aromatic Features in Emission 6.2,7.7,8.6 & 11.3 micron (Lu+03; a subsample of Dale+00) Spitzer IRAC & MIPS non-interacting Histograms: Smith+07 sample from SINGS Points Averages over parameter sets Spitzer IR Normal Galaxy Survey (SINGS ; Kennicutt+03; Dale+05) Non-tidally perturbed & non-interacting galaxies (Smith+07, a SINGS subsample & Lanz+13 from KINGFISH) HERSCHEL BANDS non-interacting Gray: Lanz+13 Color: 8 simulated galaxies, averages & dispersions over parameter sets Key Insights on Nearby Galaxies: FIR Survey w Herschel (KINGFISH, Kennicutt+11) All normal types 61 galaxies imaged with PACS and SPIRE (Dale+12) Non-tidally perturbed & non-interacting galaxies (Smith+07, a SINGS subsample & Lanz+13 from KINGFISH) UV and optical flux density ratios Non-interacting Gray: data Dale+07 Color: 8 simulated galaxies, averages & dispersions over parameter sets GRASIL-3D DISCUSSION Find encouranging results when comparing with disk galaxies in detail Changing rho_mc_thres and PDF sig Parameter variations: not remarkable effects when kept within their ranges II IR-submm EMISSION from DWARF GALAXIES The CLUES project LOCAL GROUP (Isabel Santos +, in prep) THE CLUES PROJECT CLUES: Constrained I.C. (Hoffman +Ribak 92) ** Observational data imposed as constraints on the IC → local Universe skeleton at Mpc ** Random at sub-Mpc SIMULATION: GASOLINE LCDM Grav.softening = 220 pc m_DM, m_*, m_gas 30, 2, 6 x10^4 M_sun Feedback ERIS simulation (Guedes+11) Includes chemical evolution RESULTS: Luminosity – color BLUE, CYAN: SF dwarfs RED: ¨dead¨ dwarfs Data from Mateo 1998 some relations Iron vs luminosity Black Simulated D galaxies Red Data McConnachie+12 Dwarfs are low Z systems RESULTS: velocity disp. vs M_* RESULTS: half-light radii vs M_V RESULTS: SEDs for low M* & Z SF galaxies Simulations + GRASIL → Two dust components, as observations demand Galametz+09 RESULTS: Irr low M* SF galaxy Ks FUV MIPS160 SFRH SPIRE500 III GRASIL-3D as a test bed for MASS and SFRH DETERMINATION in SPIRAL GALAXIES Obreja et al., 14 MAGICC Project, Brook & Stinson 2012 Www.star.uclan.ac.uk/Cbb/magicc MOTIVATION Constraining galaxy formation scenarios through MS: correlation SFR vs M_* MZ: M_* vs metallicities (Wuyts + 11) Gas phase Stars (Garnett + 02; Tremonti + 04) (Cowie & Berger 08; Pérez-Montero + 09) Projections of a fundamental relation? Ellison +08 COMPARING SIMU OUTPUTS TO OBSERVATIONAL DATA OBSERVATIONS: M_* & SFR determined from light (SEDs) SIMULATIONS: need to apply the same recipees !! NEED SEDS as close to observed ones as possible SOFTWARE TELESCOPES Figure 1 from Galaxy Structure and Mode of Star Formation in the SFR-Mass Plane z ~ 2.5 to z ~ 0.1 Stijn Wuyts et al. 2011 Constant slope Zero point ---> high-z galaxies form stars faster than local ones with same M_* Scatter independent of z Increases at lower M_* SIMULATIONS METHODS Disk gal. from the MaGICC project (Brook + 12; Stinson + 13) GRASIL-3D post-processing Face-on SB in r-band ----> Petrosian radii R_p (Blanton + 01) ** Luminosities, fluxes & colors from SEDs within 2R_p ready to apply observational techniques including dust effects MIMIC OBSERVATIONS ¨observed¨as they evolve from z=3.5 upto z=0 (324 snapshots) METHODS STELLAR MASS DETERMINATION Color dependent mass-to-light relations B- and V-band (McGaugh et al. in prep) GLOBAL SFR IR-corrected far UV tracer of Hao + 11: FUV flux corrected using the total IR emission WARNING Test that simulated galaxy ** B-V and M_V are within those of the sample used for calibration ** IRX vs FUV -NUV used for calibration RESULTS: M_* Testing observational methods M_* assembly history, scatter is shown Black: as predicted by simulations Blue: B-band mass-to-light ratios Green: V-band RESULTS: THE GLOBAL SFRH ¨Observational¨ SFRs vs real ones OK BLACK: SFRHs predicted by simulations BLUE: SFRHs from IR-corrected FUV RESULTS: SCATTER IN THE MS Independent of redshift Decreases with increasing M_* May trust simulations !! ---> Reflects bursting/variable SFR in the SF population RESULTS: THE FUNDAMENTAL METALLICITY RELATION M_* - SFR – (O/H) in gas (Lara-López + 10) ** ** ** ** Tight correlation Same scatter as obs Same coefficients 0.09 dex lower normalization GREY POINTS: simulated at z<3.5 RED POINTS: simulations in equally populated M_* bins BLUE LINES: solid - linear fit with slope 1, as in Lara-López + 10 Dashed – 0.16 dex scatter BLACK LINES: solid & dashed - fit Lara-López data & scatter CONCLUSIONS APPLICATION III GRASIL-3D METHOD to test out the observational methods to determine M_* and the SFRH in star forming galaxies Consistency observations -simulations The MS and MZ relation for star forming galaxies Are projections of the Fundamental Plane M_*-SFR-O/H (Mannucci+ 10; Lara-López+ 10) Prediction: the FP holds also for lower M_* starforming galaxies GENERAL CONCLUSIONS GRASIL-3D particular strengths follow GRASIL (Silva+ 98; 99) General applicability to systems with arbitrary geometry, in particular those produced in hydrodynmical simulations (evolutionary history, SFRH ..) Subresolution PDF formalism to describe MC/cirrus density field Comparison to observations of local galaxy samples are encouraging, particularly remarkable for PAH features Detailed analysis of parameter space from literature gives consistent results Many specific applications possible: different predictions on individual & statistical galaxy properties, directly comparable to observations Applications so far give encouraging results STAR FORMATION d rho_g/dt = - e_ff rho_g/t_ff , rho_g>rho_t (K-S-like) A few parsec resolution Sne II E_II = 10^51 (mass/10 M_sun) erg injected in the ISM after 10 Myear a 8 – 40 M_sun star is formed Sne Blast wave in adiabatic expansion if parsec-scale resolution (McKee & Ostriker 1977; Stinson et al. 2006; Brook 2010 . 2011) SnIa E_I = E_II, but with slower timescale + metals UNRESOLVED ISM (a few 100 pc for discs) mimic through tuning resolved physics: H_2 formation, small-scale turbulence, radiative effects free parameters, based upon core-scale physics : stocastic model (Katz 1992; parameter testing in Agertz et al. 2011) RESULTS: SOME IMAGES FUV, Ks, SPIRE 500 SFRH SNE BLAST WAVE MODEL ** Sne explosions large volumes of hot, low-densitygas McKee & Ostriker analytical blast wave model ** Mimic its effect in SPH codes: Sne feedback from m_* >8M_o (Thacker & Couchman 2000; Stinson et al. 2006; Brook et al. 2011) Energy from massive stars prior to their explosions (Stinson+ 13) weak coupling of stellar energy to the sorrounding gas 1% Flow outwards + SFR regulated GASOLINE RUNS: 3 galaxies m_bar = 2 and 0.25 x 10^5 M_o e_g = 312,5 pc - 156,2 pc M_* = 2.3 - 0.6 x 10^10 M_o Disk & bulge scales, kine, B/D consistent with observations